Numerical simulations rapidly became an efficient tool to understand the
different physical processes at work in the circumstellar medium of massive
stars [1]}, [2]}, [3]}, [4]}, [5]}, [6]}, [7]},
to constrain stellar evolution models/probe local ISM
conditions [8]}, [9]},
and to understand the pre-supernova surroundings of dying massive
stars, with which supernovae shock waves subsequently
interact [10]}, [11]}, [12]}, [13]}, [14]}.
Particularly, the gas nebulae formed around Wolf-Rayet stars have been
studied numerically as evolved winds, colliding with the material of a
larger-scale main-sequence wind-blown bubble [15]}, [16]}, [17]}, [18]}.
